论文标题
中子星合并中密度振荡的散装粘性阻尼
Bulk Viscous Damping of Density Oscillations in Neutron Star Mergers
论文作者
论文摘要
在本文中，我们讨论了与中子星星合并有关的温度范围内密度振荡的阻尼。这种阻尼是由于弱相互作用``urca''过程的中子衰变和电子捕获过程引起的。核物质是在相对论密度功能方法中建模的。散装粘度达到了接近中微子捕获温度的谐振最大值，然后随着温度升高到中微子被困在中子恒星中的范围内迅速下降。我们研究了合并后对象中的散装粘性耗散时间尺度，并确定这些时间表与特征时间尺度$ \ sim $ 10毫秒的短距离，因此可能会影响合并后对象的演变。我们的分析表明，在不太高的几个MEV和密度达到几次饱和密度时，大量粘性阻尼至关重要。
In this paper, we discuss the damping of density oscillations in dense nuclear matter in the temperature range relevant to neutron star mergers. This damping is due to bulk viscosity arising from the weak interaction ``Urca'' processes of neutron decay and electron capture. The nuclear matter is modelled in the relativistic density functional approach. The bulk viscosity reaches a resonant maximum close to the neutrino trapping temperature, then drops rapidly as temperature rises into the range where neutrinos are trapped in neutron stars. We investigate the bulk viscous dissipation timescales in a post-merger object and identify regimes where these timescales are as short as the characteristic timescale $\sim$10 ms, and, therefore, might affect the evolution of the post-merger object. Our analysis indicates that bulk viscous damping would be important at not too high temperatures of the order of a few MeV and densities up to a few times saturation density.
